J/ApJ/833/178 GLASS. VII. Hα maps (Vulcani+, 2016)
The Grism Lens-Amplified Survey from Space (GLASS).
VII. The diversity of the distribution of star formation in cluster and
field galaxies at 0.3≤z≤0.7.
Vulcani B., Treu T., Schmidt K.B., Morishita T., Dressler A.,
Poggianti B.M., Abramson L., Bradac M., Brammer G.B., Hoag A., Malkan M.,
Pentericci L., Trenti M.
<Astrophys. J., 833, 178-178 (2016)>
=2016ApJ...833..178V 2016ApJ...833..178V (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts ; Equivalent widths ;
Photometry, H-alpha
Keywords: galaxies: clusters: general; galaxies: evolution; galaxies: formation;
galaxies: general; galaxies: star formation
Abstract:
Exploiting the slitless spectroscopy taken as part of the Grism
Lens-Amplified Survey from Space (GLASS), we present an extended
analysis of the spatial distribution of star formation in 76 galaxies
in 10 clusters at 0.3<z<0.7. We use 85 foreground and background
galaxies in the same redshift range as a field sample. The samples are
well matched in stellar mass (108-1011M☉) and star formation
rate (0.5-50M☉/yr). We visually classify galaxies in terms of
broad band morphology, Hα morphology, and likely physical
process acting on the galaxy. Most Hα emitters have a spiral
morphology (41%±8% in clusters, 51%±8% in the field), followed by
mergers/interactions (28%±8%, 31%±7%, respectively) and early-type
galaxies (remarkably as high as 29%±8% in clusters and 15%±6% in
the field). A diversity of Hα morphologies is detected,
suggesting a diversity of physical processes. In clusters, 30%±8% of
the galaxies present a regular morphology, mostly consistent with star
formation diffused uniformly across the stellar population (mostly in
the disk component, when present). The second most common morphology
(28%±8%) is asymmetric/jellyfish, consistent with ram-pressure
stripping or other non-gravitational processes in 18%±8% of the
cases. Ram-pressure stripping appears significantly less prominent in
the field (2%±2%), where the most common morphology/mechanism
appears to be consistent with minor gas-rich mergers or clump
accretion. This work demonstrates that while environment-specific
mechanisms affect galaxy evolution at this redshift, they are diverse
and their effects are subtle. A full understanding of this complexity
requires larger samples and detailed and spatially resolved physical
models.
Description:
The Grism Lens-Amplified Survey from Space (GLASS) is a 140 orbit
slitless spectroscopic survey conducted with HST in cycle 21. It has
observed the cores of 10 massive galaxy clusters with the WFC3 NIR
grisms G102 and G141 providing an uninterrupted wavelength coverage
from 0.8um to 1.7um. The 10 clusters are listed in Table 1.
Observations for GLASS were completed in 2015 January.
Building on our pilot study presented in Vulcani+ (2015ApJ...814..161V 2015ApJ...814..161V),
we have continued our exploration of the spatial distribution of star
formation in galaxies at 0.3≤z≤0.7, as traced by the Hα
emission in the field of view of the 10 GLASS clusters, detailing and
strengthening our previous results. We have produced Hα maps,
taking advantage of the HST/WFC3 G102 and WFC3-G141 data at two
orthogonal position angles.
In a companion paper (Paper VIII; Vulcani+ 2017ApJ...837..126V 2017ApJ...837..126V), we
investigate trends with cluster properties, such as the hot gas
density as traced by the X-ray emission, the total surface mass
density as inferred from gravitational lens models, and the local
number density, to inspect whether or not local cluster conditions
have an impact on the extent and location of the star formation.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 99 10 Cluster properties
table3.dat 262 162 Properties of galaxies
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See also:
J/A+A/590/A31 : ASTRODEEP Frontier Fields Catalogues (Merlin+, 2016)
J/ApJ/831/182 : GLASS. VI. MCS J0416.1-2403 HFF imaging + spectra (Hoag+, 2016)
J/AJ/151/78 : Jellyfish galaxy cand. in galaxy clusters (Poggianti+, 2016)
J/ApJ/812/114 : Grism Lens-Amplified Survey from Space (GLASS) I. (Treu+, 2015)
J/ApJ/811/29 : GLASS. IV. Lensing cluster Abell 2744 (Wang+, 2015)
J/MNRAS/452/1437 : Abell 2744 strong-lensing analysis (Jauzac+, 2015)
J/MNRAS/446/3943 : galaxies 2D phot. decompositions in SDSS-DR7 (Meert+, 2015)
J/MNRAS/440/843 : SIM2D parameters of SDSS-DR7 galaxies (Omand+, 2014)
J/ApJS/211/21 : Spectroscopic redshifts of galaxies in MACS (Ebeling+, 2014)
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
J/AJ/141/14 : HST WFC3 ERS : emission-line galaxies (Straughn+, 2011)
J/ApJ/633/174 : Spheroidals and bulge dominated galaxies (Treu+, 2005)
http://glass.astro.ucla.edu/ : GLASS home page
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Cluster Name
17- 24 A8 --- Cl Shortened cluster name used in article
26- 27 I2 h RAh Hour of Right Ascension (J2000)
29- 30 I2 min RAm Minute of Right Ascension (J2000)
32- 35 F4.1 s RAs Second of Right Ascension (J2000)
37- 37 A1 --- DE- Sign of the Declination (J2000)
38- 39 I2 deg DEd Degree of Declination (J2000)
41- 42 I2 arcmin DEm Arcminute of Declination (J2000)
44- 47 F4.1 arcsec DEs Arcsecond of Declination (J2000)
49- 53 F5.3 --- z [0.3/0.7] Redshift
55- 59 F5.3 kpc/arcsec Scale [4.5/7.1] Physical scale of observations
61- 65 F5.2 10+37W Lx [8/47.4] X-ray luminosity
67- 70 F4.2 10+37W e_Lx [0.3/1.6] Uncertainty for Lx
72- 76 F5.2 10+14Msun M500 [6.6/25] Virial Mass from Mantz+
(2010MNRAS.406.1773M 2010MNRAS.406.1773M)
78- 81 F4.2 10+14Msun e_M500 [0.8/3.3] Uncertainty in M500
83- 86 F4.2 Mpc r500 [1/1.8] Virial Radius
88- 91 F4.2 Mpc e_r500 [0.05/0.09] Uncertainty in r500
93- 95 I3 deg PA1 [8/203] Position Angle 1
97- 99 I3 deg PA2 [88/328] Position Angle 2
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Cl Shortened cluster name used in article
9- 13 I05 --- Name [00063/03965] Galaxy Name
15- 26 F12.8 deg RAdeg Right Ascension (J2000)
28- 40 F13.9 deg DEdeg Declination (J2000)
42- 48 F7.5 --- z [0.2/0.8] Redshift (1)
50- 56 F7.4 mag mag [17.5/25.7] Magnitude, AB magnitude
(MAG-AUTO)
58- 65 F8.2 [Msun] logMass [7/11.3]?=-9999 Log mass
67- 73 F7.1 0.1nm EW [-1061/422] Hα equivalent width
75- 81 F7.1 0.1nm e_EW [-1302/447] Uncertainty in EW
83-101 F19.13 Msun/yr SFR [0.03/180]?=-9999 Star formation rate
103-121 F19.13 Msun/yr e_SFR [0.04/6]?=-9999 Uncertainty in SFR
123-142 F20.14 Msun/yr/kpc2 SigSFR [0.004/3.6]?=-9999 Star formation
density
144-163 F20.14 Msun/yr/kpc2 e_SigSFR [0.003/0.08]?=-9999 Uncertainty in
SFR-den
165-183 F19.13 kpc offsetPA1 [/1.4]?=-9999 Hα Offset 1 (2)
185-203 F19.13 kpc e_offsetPA1 [0/2]?=-9999 Uncertainty in offsetPA1
205-223 F19.13 kpc offsetPA2 [-2.7/2.8]?=-9999 Hα Offset 2 (2)
225-243 F19.13 kpc e_offsetPA2 [-1.6/1]?=-9999 Uncertainty in
offsetPA2
245-249 A5 --- Vis Broad-band continuum morphology (3)
251-256 A6 --- Ha Hα morphology (4)
258-262 A5 --- Hap Main processes acting on the galaxy (5)
--------------------------------------------------------------------------------
Note (1): Redshifts slightly changed from the GLASS catalog to better match
the center of the Hα maps.
Note (2): Offsets between the Hα emission and the continuum emission
(as measured form the F475W filter) along the two directions. Reported
offsets are along the y-direction of the corresponding position angle
(see table 1). The orientation of the offset (counterclockwise from North)
is θ=-PA1-44.69.
Note (3): Broad-band continuum morphologies as follows:
Ell = Elliptical (28 occurrences);
S0 = Lenticular (7 occurrences);
Spir = Spiral (74 occurrences);
Irr = Irregular (4 occurrences);
Mer = Merger (47 occurrences).
Note (4): Hα morphologies as follows:
Reg = Regular (40 occurrences);
Clumpy = Clumpy (53 occurrences);
Conc = Concentrated (27 occurrences);
Asy = Asymmetric/jellyfish (41 occurrences).
Note (5): Main processes acting on the galaxy as follows:
Reg = nothing; when the Hα light distribution appears regular and
undisturbed (57 occurrences);
RP = ram pressure stripping (19 occurrences);
MaM = Major Merger (25 occurrences);
MiM = Minor Merger/interaction, when the F475W filter shows the presence
of material infalling onto the main galaxies that is not detected
in the F140W filter, suggesting a low mass-to-light ratio and a
low stellar mass (50 occurrences);
other = other (10 occurrences).
See section 3.6 for further details.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Treu et al. Paper I. 2015ApJ...812..114T 2015ApJ...812..114T Cat. J/ApJ/812/114
Jones et al. Paper II. 2015AJ....149..107J 2015AJ....149..107J
Schmidt et al. Paper III. 2016ApJ...818...38S 2016ApJ...818...38S
Wang et al. Paper IV. 2015ApJ...811...29W 2015ApJ...811...29W Cat. J/ApJ/811/29
Vulcani et al. Paper V. 2015ApJ...814..161V 2015ApJ...814..161V
Hoag et al. Paper VI. 2016ApJ...831..182H 2016ApJ...831..182H Cat. J/ApJ/831/182
Vulcani et al. Paper VII. 2016ApJ...833..178V 2016ApJ...833..178V This catalog.
Vulcani et al. Paper VIII. 2017ApJ...837..126V 2017ApJ...837..126V
Morishita et al. Paper IX. 2017ApJ...835..254M 2017ApJ...835..254M Cat. J/ApJ/835/254
Wang et al. Paper X. 2017ApJ...837...89W 2017ApJ...837...89W
Schmidt et al. Paper XI. 2017ApJ...839...17S 2017ApJ...839...17S
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-Apr-2017